To our knowledge, O i \(\) 8446 was not observed during the HST monitoring but it has been observed at other times. [1]} give average fluxes for O i \(\) 8446 and H\(\)  from high-quality spectra obtained on three nights in May 2004, January 2006, and June 2006. These give an O i \(\) 8446/H\(\)  ratio of = 0.16. Earlier but lower-quality observations of [2]} gave a similar ratio of 0.18. The relative strength of O i \(\) 8446 compared with H\(\)  in NGC 5548 is very close to the median relative strength in other AGNs (see Table 1 of [2]}). The O i \(\) 8446/H\(\)  ratio of [1]} and the O i \(\) 1304/H\(\)  ratio during the 1993 monitoring (see Figure 5) give an O i \(\) 1304/\(\) 8446 ratio of \(1.375 \pm 0.08\) . This gives \(E(1304-8446) = 1.68 \pm 0.13\)  magnitudes.
